We are an active grouping of almost 20 members, including academics, researchers and postgraduate research students, based in the School of Physical Sciences. We use a range of cutting-edge laboratory instrumentation to investigate the geochemical and isotopic signatures of the dust and organic material present at the birth of the Solar System (now contained in extraterrestrial samples of cometary, asteroidal and interplanetary dust) and how this material evolved during the early stages of planetary accretion and differentiation. Our facilities include unique (e.g. high sensitivity C, N, noble gas mass spectrometer system) and world-leading (e.g. oxygen 3-isotope laser fluorination system; NanoSIMS 50L) instruments as well as many more routine instruments (e.g. Raman, analytical SEM) that permit detailed investigation of such complex materials. A major focus is on investigating the origin and distribution of the astrobiologically important light volatile elements (e.g., H, C, N, O). Most of our research is carried out in collaboration with planetary scientists, each of whom has an international reputation and is actively involved in a wide range of planetary missions such that the results from our projects contribute towards, and benefit from, recent (e.g. Stardust, Hayabusa), on-going (e.g. Rosetta) and future (e.g. OSIRIS-REx) missions.

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Potential research projects

Isotope reservoirs in the early solar system

Origin of organic matter in primitive materials

Preparation for returned samples (lunar, asteroidal)

The role of volatiles in the protoplanetary disc

Projects mainly involve detailed laboratory investigations of extraterrestrial samples using the latest generation of analytical instruments such as mass spectrometers, FIB-SEM, EPMA, Raman, NanoSIMS. Each project provides a good balance between application of existing analytical methods and development of new and innovative analytical protocols ensuring international leadership in the field of planetary geochemistry.